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Oxygen, sulfur, and...
Oxygen, sulfur, and iron radial abundance gradients of classical Cepheids across the Galactic thin disk
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- da Silva, R. (författare)
- Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Agenzia Spaziale Italiana, Space Science Data Center, via del Politecnico snc, Rome, 00133, Italy
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- D’Orazi, V. (författare)
- Department of Physics, University of Rome Tor Vergata, via della Ricerca Scientifica 1, Rome, 00133, Italy; Inaf -Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, Padova, 35122, Italy
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- Palla, M. (författare)
- Sterrenkundig Observatorium, Ghent University, Krijgslaan 281 - S9, Gent, 9000, Belgium; Inaf -Osservatorio Astronomico di Bologna, via Gobetti 93/3, Bologna, 40129, Italy
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- Bono, G. (författare)
- Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Department of Physics, University of Rome Tor Vergata, via della Ricerca Scientifica 1, Rome, 00133, Italy
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- Braga, V. F. (författare)
- Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Agenzia Spaziale Italiana, Space Science Data Center, via del Politecnico snc, Rome, 00133, Italy
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- Fabrizio, M. (författare)
- Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Agenzia Spaziale Italiana, Space Science Data Center, via del Politecnico snc, Rome, 00133, Italy
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- Lemasle, B. (författare)
- Astronomisches Rechen-Institut, Zah, Universität Heidelberg, Mönchhofstr. 12-14, Heidelberg, 69120, Germany
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- Spitoni, E. (författare)
- Inaf, Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, Trieste, 34131, Italy
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- Matteucci, F. (författare)
- Inaf, Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, Trieste, 34131, Italy; Dipartimento di Fisica, Sezione di Astronomia, Università Degli Studi di Trieste, via G. B. Tiepolo 11, Trieste, 34131, Italy; Infn, Sezione di Trieste, via A. Valerio 2, Trieste, 34100, Italy
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- Jönsson, H. (författare)
- Malmö universitet,Institutionen för materialvetenskap och tillämpad matematik (MTM)
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- Kovtyukh, V. (författare)
- Astronomical Observatory, Odessa National University, Shevchenko Park, Odessa, 65014, Ukraine
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- Magrini, L. (författare)
- Inaf -Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, Firenze, Italy
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- Bergemann, M. (författare)
- Max Planck Institute for Astronomy, Heidelberg, 69117, Germany; Niels Bohr International Academy, Niels Bohr Institute, Blegdamsvej 17, Copenhagen, 2100, Denmark
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- Dall’Ora, M. (författare)
- Inaf -Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, Napoli, 80131, Italy
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- Ferraro, I. (författare)
- Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy
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- Fiorentino, G. (författare)
- Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy
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- François, P. (författare)
- Gepi, Observatoire de Paris, Psl Research University, Cnrs, 61 avenue de l'Observatoire, Paris, 75014, France; Upjv, Université de Picardie Jules Verne, 33 rue St Leu, Amiens, 80080, France
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- Iannicola, G. (författare)
- Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy
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- Inno, L. (författare)
- Science and Technology Department, Parthenope University of Naples, Naples, Italy
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- Kudritzki, R.-P. (författare)
- Lmu München, Universitätssternwarte, Scheinerstr. 1, München, 81679, Germany; Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, 96822, HI, United States
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- Matsunaga, N. (författare)
- Department of Astronomy, School of Science, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan; Laboratory of Infrared High-Resolution Spectroscopy (LiH), Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, 603-8555, Japan
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- Monelli, M. (författare)
- Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Instituto de Astrofísica de Canarias (IAC), C. Vía Láctea s/n, La Laguna, 38205, Spain; Departamento de Astrofísica, Universidad de la Laguna (ULL), Laguna, 38200 La, Spain
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- Nonino, M. (författare)
- Inaf, Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, Trieste, 34131, Italy
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- Sneden, C. (författare)
- Department of Astronomy and McDonald Observatory, The University of Texas, Austin, 78712, TX, United States
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- Storm, J. (författare)
- Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, Potsdam, 14482, Germany
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- Thévénin, F. (författare)
- Université Côte d'Azur, Observatoire de la Côte d'Azur, Cnrs, Lagrange Umr 7293, Cs 34229 Cedex, Nice, 06304-4, France
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- Tsujimoto, T. (författare)
- National Astronomical Observatory of Japan, Mitaka, Tokyo, 1818588, Japan
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- Zocchi, A. (författare)
- Department of Astrophysics, University of Vienna, Türkenschanzstraße 17, Vienna, 1180, Austria
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(creator_code:org_t)
- EDP Sciences, 2023
- 2023
- Engelska.
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Ingår i: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 678, s. A195-A195
- Relaterad länk:
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https://doi.org/10.1...
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https://mau.diva-por... (primary) (Raw object)
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https://urn.kb.se/re...
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https://doi.org/10.1...
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Abstract
Ämnesord
Stäng
- Context. Classical Cepheids (CCs) are solid distance indicators and tracers of young stellar populations. Dating back to the beginning of the 20th century, they have been safely adopted to trace the rotation, kinematics, and chemical enrichment history of the Galactic thin disk.Aims. The main aim of this investigation is to provide iron, oxygen, and sulfur abundances for the largest and most homogeneous sample of Galactic CCs analyzed so far (1118 spectra of 356 objects). The current sample, containing 70 CCs for which spectroscopic metal abundances are provided for the first time, covers a wide range in galactocentric distances, pulsation modes, and pulsation periods.Methods. Optical high-resolution spectra with a high signal-to-noise ratio that were collected with different spectrographs were adopted to provide homogeneous estimates of the atmospheric parameters (effective temperature, surface gravity, and microturbulent velocity) that are required to determine the abundance. Individual distances were based either on trigonometric parallaxes by the Gaia Data Release 3 (Gaia DR3) or on distances based on near-infrared period-luminosity relations.Results. We found that iron and α-element radial gradients based on CCs display a well-defined change in the slope for galactocentric distances larger than ~12 kpc. We also found that logarithmic regressions account for the variation in [X/H] abundances from the inner to the outer disk. Radial gradients for the same elements, but based on open clusters covering a wide range in cluster ages, display similar trends. This means that the flattening in the outer disk is an intrinsic feature of the radial gradients because it is independent of age. Empirical evidence indicates that the S radial gradient is steeper than the Fe radial gradient. The difference in the slope is a factor of two in the linear fit (−0.081 vs. −0.041 dex kpc−1) and changes from −1.62 to −0.91 in the logarithmic distance. Moreover, we found that S (explosive nucleosynthesis) is underabundant on average when compared with O (hydrostatic nucleosynthesis). The difference becomes clearer in the metal-poor regime and for the [O/Fe] and [S/Fe] abundance ratios. We performed a detailed comparison with Galactic chemical evolution models and found that a constant star formation efficiency for galactocentric distances larger than 12 kpc accounts for the flattening observed in both iron and α-elements. To further constrain the impact of the predicted S yields for massive stars on radial gradients, we adopted a toy model and found that the flattening in the outermost regions requires a decrease of a factor of four in the current S predictions.Conclusions. CCs are solid beacons for tracing the recent chemical enrichment of young stellar populations. Sulfur photospheric abundances, when compared with other α-elements, have the key advantage of being a volatile element. Therefore, stellar S abundances can be directly compared with nebular sulfur abundances in external galaxies.
Ämnesord
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Nyckelord
- Galaxy: disk
- stars: abundances
- stars: fundamental parameters
- stars: variables: Cepheids
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- ref (ämneskategori)
- art (ämneskategori)
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da Silva, R.
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D’Orazi, V.
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Palla, M.
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Bono, G.
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Braga, V. F.
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Fabrizio, M.
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Lemasle, B.
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Spitoni, E.
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Matteucci, F.
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Jönsson, H.
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Kovtyukh, V.
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Magrini, L.
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Bergemann, M.
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Dall’Ora, M.
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Ferraro, I.
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Fiorentino, G.
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François, P.
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Iannicola, G.
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Inno, L.
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Kudritzki, R.-P.
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Matsunaga, N.
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Monelli, M.
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Nonino, M.
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Sneden, C.
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Storm, J.
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Thévénin, F.
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Tsujimoto, T.
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Zocchi, A.
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Malmö universitet